# Accretion disk around the rotating Damour-Solodukhin wormhole

## TL;DR

This paper investigates the accretion disk properties around a new rotating Damour-Solodukhin wormhole, finding that many kinematic features are identical to Kerr black holes, with subtle differences in emissivity that are currently unobservable.

## Contribution

It introduces the Kerr-like wormhole model and analyzes its accretion disk properties, revealing that many features are indistinguishable from Kerr black holes, with some differences in emissivity at high spin.

## Key findings

- Kinematic properties are independent of the wormhole parameter , matching Kerr black holes.
- Differences in emissivity appear at high  and extreme spin, but are too small to detect currently.
- Luminosity peak behaviors differ, offering potential observational signatures.

## Abstract

A new rotating generalization of the Damour-Solodukhin wormhole (RDSWH), called Kerr-like wormhole, has recently been proposed and investigated by Bueno \textit{et al} for echoes in the gravitational wave signal. We show a novel feature of the RDSWH, viz., that the kinematic properties such as the ISCO\ or marginally stable radius $r_{\text{ms}}$, efficiency $\epsilon$ and the disk potential $V_{\text{eff}}$ are \textit{independent} of $\lambda$ (which means they are identical to their KBH counterparts for any given spin). Differences however appear in the emissivity properties for higher values $0.1<\lambda\leq 1$ (say) and for the extreme spin $a_{\star}=0.998$. The kinematic and emissivity are generic properties as variations of the wormhole mass and the rate of accretion within the model preserve these properties. Specifically, the behavior of the luminosity peak is quite opposite to each other for the two objects, which could be useful from the viewpoint of observations. Apart from this, an estimate of the difference $\Delta_{\lambda}$ in the maxima of flux of radiation $F(r)$ shows non-zero values but is too tiny to be observable at present for $\lambda < 10^{-3}$ permitted by the strong lensing bound. The broad conclusion is that RDSWH\ are experimentally indistinguishable from KBH by accretion characteristics.